Abstract
In the present work, we study the consequences of a recently proposed polynomial inflationary potential in the context of the generalized, modified, and generalized cosmic Chaplygin gas models. In addition, we consider dissipative effects by coupling the inflation field to radiation, i.e., the inflationary dynamics is studied in the warm inflation scenario. We take into account a general parametrization of the dissipative coefficient Gamma for describing the decay of the inflaton field into radiation. By studying the background and perturbative dynamics in the weak and strong dissipative regimes of warm inflation separately for the positive and negative quadratic and quartic potentials, we obtain expressions for the most relevant inflationary observables as the scalar power spectrum, the scalar spectral, and the tensor-to-scalar ratio. We construct the trajectories in the n_mathrm{s}–r plane for several expressions of the dissipative coefficient and compare with the two-dimensional marginalized contours for (n_mathrm{s},r) from the latest Planck data. We find that our results are in agreement with WMAP9 and Planck 2015 data.
Highlights
In the slow-roll period the universe undergoes an accelerated expansion as the potential energy of the inflaton field dominates over its kinetic energy and all interactions of the inflaton scalar field with other field degrees of freedom are typically neglected
The kinetic energy of the inflaton field becomes comparable to its potential energy, and by transferring its energy to massless particles it oscillates around the minimum of the potential
The main goal of the present paper is to study the consequences of considering a polynomial inflationary potential in the context of the generalized, modified, and generalized cosmic Chaplygin gas models
Summary
In the slow-roll period the universe undergoes an accelerated expansion as the potential energy of the inflaton field dominates over its kinetic energy and all interactions of the inflaton scalar field with other field degrees of freedom are typically neglected. The universe is filled with relativistic particles and the universe enters in the radiation big-bang epoch There is another dynamical mechanism for obtaining a successful slow-roll inflation, i.e., the warm inflation scenario [9,10,11,12,13]. Linde [14] introduced the concept of chaotic inflation in order to interpret the initial conditions for scalar field driving inflation which may help in solving the persisting problems of the old inflation models In this model, the inflaton potential was chosen to be quadratic or quartic form, i.e. Panotopoulos and Videla [27] discussed warm inflation by assuming the quartic potential and an inflaton decay rate proportional to the temperature and found that their results are in agreement with the latest Planck data, obtaining a lower value for the tensor-to-scalar ratio compared to the cold inflation scenario.
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